Dark Matter in Astro- and Particle Physics: Proceedings of by Luigi Guzzo (auth.), Professor Dr. H. V.

By Luigi Guzzo (auth.), Professor Dr. H. V. Klapdor-Kleingrothaus, Professor Dr. R. D. Viollier (eds.)

The look for darkish subject within the Universe has confirmed itself as some of the most interesting and valuable fields of astrophysics, particle physics and cosmology. The lectures and talks during this e-book emphasize the experimental and theoretical prestige and destiny views, stressing specifically the interaction among astro- and particle physics.

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Extra resources for Dark Matter in Astro- and Particle Physics: Proceedings of the International Conference DARK 2002, Cape Town, South Africa, 4–9 February 2002

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The central filled dashed circle marks the radio position of SgrA * and corresponding uncertainties of ±30 mas. 4% and from the thick contour line at the 90% level. The time averaged positions of the SHARP /NTT and NIRC/Keck data as well as the error cones of the acceleration data for Sl and S2 are indicated by different symbols explained in the figure legend. The positional uncertainties for the SHARP and NIRC positions have been included in the grey scale plot and the width of the cones. Eckart & Straubmeier 21 S2, and S8.

498-503 Dim Matter in the Disks of Low Surface Brightness Galaxies Burkhard Fuchs Astronomisches Rechen-Institut, 69120 Heidelberg, Germany Abstract. An attempt is made to set constraints on the otherwise ambiguous decomposition of the rotation curves of low surface brightness galaxies into contributions due to the various components of the galaxies. For this purpose galaxies are selected which show clear spiral structure. Arguments of density wave theory of galactic spiral arms are then used to estimate the masses of the galactic disks.

From Sgr A* assuming (physically not realistic) Plummer like density distributions (see discussion in Genzel et al. 1996, 2000) with a core radius Tc and a mass density p(O) at the very center of the distribution. We chose the exponent a=5, since this corresponds to the steepest currently observed drop in cluster mass density. For the stars SI and S2 which are currently closest in projection to Sgr A* the mean value and error of the enclosed mass corrected for a volume radius of about 15 mpc is Mace = (5 ± 3) X 106 M0 .

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